News Release Archive:

News Release 782 of 1051

February 10, 1998 12:00 AM (EST)

News Release Number: STScI-1998-08

Shock Wave Sheds New Light on Fading Supernova

Background information useful for exploring this news release:

Diary of a Supernova: Key Events in the History of Sn1987a

February 23, 1987: Canadian astronomer Ian Shelton at Las Campanas Observatory in Chile takes a telescopic photo of a small galaxy 167,000 light-years from Earth called the Large Magellanic Cloud. For Shelton, it is just routine work - until he develops the photographic plate. On that plate, he notices an extremely bright star, an intruder that he had not seen in previous observations of the same area. He races outside and looks up at the sky. There it is: a star of about the fifth magnitude, glowing in the sky. He realizes this "new star" actually is an aging massive star that has blown itself apart in a supernova explosion. (The star actually blew up about 165,000 BC, but its light arrived here in 1987.)

Astronomers are excited with this discovery because it is the nearest supernova in 400 years, since Johannes Kepler observed one in our Milky Way Galaxy in 1604.

Data taken by a small telescope aboard the International Ultraviolet Explorer (IUE) satellite help astronomers identify the exploding star's location as Sanduleak -69 degrees 202, the former site of a blue supergiant about 20 times the mass of the Sun. Astronomers name the exploding star supernova 1987A.

Astronomers believe the star swelled up to become a red supergiant, puffed away some mass, then contracted and reheated to become a blue supergiant. Then, in less than a second, the star's core collapsed, and a wave of neutrinos heated the inner core to 10 billion degrees Fahrenheit. This process triggered a shock wave that ripped the star apart, propelling a burst of neutrinos - ghostly particles from the star's core - into space.

The neutrinos are picked up by deep underground detectors: the IMB detector in Ohio and Kamiokande II in Japan. These invisible particles are the first signal of the supernova explosion, arriving even before the bright light from the dying star.

May 1987: IUE discovers an abundance of chemical elements in the supernova debris, an indicator that the progenitor star had already passed through the red giant phase.

July 1987: The Japanese satellite GINGA and a West German X-ray telescope called HEXE, attached to the Soviet Mir space station, detect X-rays emanating from the supernova debris.

August to November 1987: Several research missions, including the Solar Maximum Satellite, detect high-energy gamma rays - released in the decay of radioactive elements formed in nuclear reactions at the core of the dying star. The data show that the explosion created from simple building blocks a multitude of chemical elements. Among them was radioactive nickel, which decays into cobalt, which rapidly transforms into stable iron. The discovery confirms a widely held theory that supernovas produce the heavy chemical elements that make up most things on Earth.

December 1989: Optical observations by the European Southern Observatory's New Technology Telescope in La Silla, Chile, show a bright doughnut or ring-like feature around the supernova.

August 1990: The Faint Object Camera, an instrument aboard the newly deployed Hubble Space Telescope, clearly shows a narrow ring around the supernova. The distance between the ring and the supernova is about three-quarters of a light-year. Astronomers believe this ring was formed before the supernova explosion, ejected by the blue supergiant star about 20,000 years before its violent demise.

1990: Rapidly brightening radio emissions are detected by the Australia Telescope National Facility. (Radio waves were detected for two weeks after the supernova was first spotted.) Astronomers determine that the radio waves are coming from an area that lies between the ring and the glowing debris of the supernova at the center of the ring. In that region, the most rapidly moving debris of the supernova is crashing into gas. Optical telescopes cannot detect the gas because its density is too low and its temperature is too high.

1992: The NASA-Germany ROSAT satellite detects rapidly brightening X-rays from the supernova. The X-rays evidently are coming from the same collision area as the radio waves.

May 1994: The Hubble telescope's Wide Field and Planetary Camera 2 (WFPC2) shows that two outer loops of glowing gas, first identified several years earlier in ground-based images, are surprisingly thin. Puzzled by Hubble's unexpected new details, astronomers are challenged to explain the processes which formed such unusual structures.

January 1997: WFPC2 shows a dumbbell-shaped structure one-tenth of a light-year long. The structure consists of two blobs of debris in the center of the supernova racing away from each other at nearly 6 million mph.

May 1997: The Hubble telescope's Space Telescope Imaging Spectrograph (STIS) produces a detailed ultraviolet image of the inner ring, identifying specific gases such as oxygen, nitrogen and hydrogen, and sulfur. By dismantling the ring into its component elements, astronomers hope to assemble a picture of how the ring was created.

June 1997: Astronomers measure the fast-moving gas ejected by the supernova explosion as it crashes into gas expelled by the progenitor star about 20,000 years before its demise. This gas was invisible until observed in ultraviolet light by STIS. The spectrograph detects the presence of glowing hydrogen expanding at a speed of 33 million mph inside the inner ring.

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